The AAO/UKST SuperCOSMOS Hα survey

Parker, Quentin A.; Phillipps, Steven; Pierce, Michael; Hartley, M.; Hambly, N. C.; Read, M.; MacGillivray, H. T.; Tritton, S. B.; Cass, C. P.; Cannon, R. D.; Cohen, Martin; Drew, J. E.; Frew, David J.; Hopewell, Ella C.; Mader, Stacy; Malin, D. F.; Masheder, M. R. W.; Morgan, D. H.; Morris, Rhys; Russeil, D.; Russell, Ken; Walker, Russell

doi:10.1111/j.1365-2966.2005.09350.x

Cited by 311 publications

(282 citation statements)

References 63 publications

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“…16). Our predicted maximum Hα emission is above the diffuse emission sensitivity limit of the SuperCOSMOS H-alpha Survey (SHS Parker et al 2005) of 1.1−2.8 × 10 −17 erg s −1 cm −2 arcsec −2 , e.g. our model OSNR4040 has a maximum emission larger than 9 × 10 −16 erg s −1 cm −2 arcsec −2 (Fig.…”

Section: Emission Mapsmentioning

confidence: 99%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before expanding into the local interstellar medium (ISM). We investigate whether the initial mass and space velocity of these progenitors can be associated with asymmetric supernova remnants. We run hydrodynamical models of supernovae exploding in the pre-shaped medium of moving Galactic core-collapse progenitors. We find that bow shocks that accumulate more than about 1.5 M ⊙ generate asymmetric remnants. The shock wave first collides with these bow shocks 160 − 750 yr after the supernova, and the collision lasts until 830 − 4900 yr. The shock wave is then located 1.35 − 5 pc from the center of the explosion, and it expands freely into the ISM, whereas in the opposite direction it is channelled into the region of undisturbed wind material. This applies to an initially 20 M ⊙ progenitor moving with velocity 20 km s −1 and to our initially 40 M ⊙ progenitor. These remnants generate mixing of ISM gas, stellar wind and supernova ejecta that is particularly important upstream from the center of the explosion. Their lightcurves are dominated by emission from optically-thin cooling and by X-ray emission of the shocked ISM gas. We find that these remnants are likely to be observed in the [OIII] λ 5007 spectral line emission or in the soft energy-band of X-rays. Finally, we discuss our results in the context of observed Galactic supernova remnants such as 3C391 and the Cygnus Loop.

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Section: Emission Mapsmentioning

confidence: 99%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…About 2700 PNe have been detected so far in the Galaxy, including the objects listed by Acker et al (1994Acker et al ( , 1996 and the new PNe found in the Southern Hemisphere by the AAO-UKST Hα survey (Parker et al 2005;Miszalski et al 2008). However, the expected Galactic PN population is much larger, with estimates varying from 28000±5000 based on observations ) to 46000 ± 13000 PNe (of size <0.9 pc) derived from stellar population synthesis models (Moe & De Marco 2006).…”

Section: Introductionmentioning

confidence: 99%

Candidate planetary nebulae in the IPHAS photometric catalogue

Viironen¹,

Greimel

Corradi³

et al. 2009

A&A

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Context. We have carried out a semi-automated search for planetary nebulae (PNe) in the INT photometric H-alpha survey (IPHAS) catalogue. We present the PN search and the list of selected candidates. We cross correlate the selected candidates with a number of existing infrared galactic surveys in order to gain further insight into the nature of the candidates. Spectroscopy of a subset of objects is used to estimate the number of PNe present in the entire candidate list. Aims. The overall aim of the IPHAS PN project is to carry out a deep census of PNe in the northern Galactic plane, an area where PN detections are clearly lacking. Methods. The PN search is carried out on the IPHAS photometric catalogue. The candidate selection is based on the IPHAS and 2MASS/UKIDSS colours of the objects and the final candidate selection is made visually. Results. From the original list of ∼600 million IPHAS detections we have selected a total of 1005 objects. Of these, 224 are known objects, leaving us with 781 PN candidates. Based on the initial follow-up spectroscopy, we expect the list to include very young and proto-PNe in addition to genuine, normal PNe (∼16%) and emission line objects other than PNe. We present additional criteria to select the most probable PN candidates from our candidate list.

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“…A significant number (∼1200) of newly discovered PNe have been listed in the Macquarie/AAO/Strasbourg Hα PNe (MASH) PN catalogues (Miszalski et al 2008;Parker et al 2006) which are a direct product of the Anglo-Australian Observatory/UK Schmidt Telescope (AAO/UKST) Hα survey (Parker et al 2005). A significant fraction of MASH PNe represent the oldest stages of PN evolution, dominating the known population at the faint end of the PN luminosity function.…”

Section: Introductionmentioning

confidence: 99%

A pilot study of the radio‐continuum emission from MASH planetary nebulae

et al. 2011

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Key words astronomical data bases: miscellaneous -planetary nebulae: general -radiation mechanisms: thermal -radio continuum: ISM We report an Australia Telescope Compact Array (ATCA) radio-continuum observations of 26 planetary nebulae (PNe) at wavelengths of 3 and 6 cm. This sample of 26 PNe were taken from the Macquarie/AAO/Strasbourg Hα PNe (MASH) catalogue and previous lists. We investigate radio detection quality including measured and derived parameters for all detected or marginally detected PNe from this combined sample. Some 11 objects from the observed sample have been successfully detected and parametrized. Except for one, all detected PNe have very low radio surface brightnesses. We use a statistical distance scale method to calculate distances and ionised masses of the detected objects. Nebulae from this sample are found to be large (>0.2 pc in diameter) and highly diluted which indicates old age. For 21 PNe from this sample we list integrated Hα fluxes and interstellar extinction coefficients, either taken from the literature or derived here from the Balmer decrement and radio to Hα ratio methods. Finally, our detected fraction of the MASH pilot sample is relatively low compared to the non-MASH sub-sample. We conclude that future radio surveys of the MASH sample must involve deeper observations with better uv coverage in order to increase the fraction of detected objects and improve the quality of the derived parameters.

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The AAO/UKST SuperCOSMOS Hα survey

Cited by 311 publications

References 63 publications

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Candidate planetary nebulae in the IPHAS photometric catalogue

A pilot study of the radio‐continuum emission from MASH planetary nebulae

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